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Mutual Phenomena of Jovian Satellites

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Mutual Phenomena of Jovian Satellites J. Astrophys. Astr. (1991) 12, 69–87 Mutual Phenomena of Jovian Satellites R. Vasundhara Indian Institute of Astrophysics, Bangalore 560034 Received 1990 September 20; accepted 1990 December 22 Abstract. Results of the observations of mutual eclipses of Galilean satellites observed from the Vainu Bappu Observatory during 1985 are presented. Theoretical models assuming a uniform disc, Lambert’s law and Lommel-Seeliger’s law describing the scattering characteristics of the surface of the eclipsed satellite were used to fit the observations. Light curves of the 1E2 event on 1985 September 24 and the 3E1 event on 1985 October 24 observed from VBO and published light curves of the 1E2 event on 1985 September 14, the 3E1 event on 1985 September 26 and the 2E1 event on 1985 October 28 (Arlot et al 1989) were fitted with theoretical light curves using Marquardt’s algorithm. The best fitting was obtained using Lommel-Seeliger’s law to describe the scattering over the surface of Iο and Europa. During the fitting, a parameter δxshift which shifts the theoretical light curve along the direction of relative motion of the eclipsed satellite with respect to the shadow centre, on the sky plane (as seen from the Sun) was determined along with the impact parameter. In absence of other sources like prominent surface features or non perfect sky conditions which could lead to asymmetric light curves, δxshift would be a measure of the phase correction (Aksnes, Franklin & Magnusson 1986) with an accuracy as that of the midtime. Heliocentric Δα cos (δ) and Δδ at mid times derived from fitted impact parameters are reported. Key words: Jupiter’s satellites—mutual phenomena, scattering character- istics—phase corrections 1. Introduction The transit of Jupiter through the nodes of its equator on its orbit twice during its orbital period of 11.6 yr, provides the opportunity for an edge-on view of its equatorial plane from the inner solar system. Inclination of the orbital planes of the Galilean satellites to the planet’s equator is very small, therefore for a few months around the time of nodal crossing, the satellites frequently eclipse or occult each other when any two of them are aligned with the Sun or Earth respectively. Observations of the mutual events provide means of observing positions of the satellites with an accuracy at least two orders of magnitude better than the photo- graphic or eclipse (behind the planet) observations. The first observations of mutual phenomena were made in 1973 (Aksnes & Franklin 1976; Arlot, Camichel & Link 1974). The mutual phenomena in 1979 (Arlot 1982) and in 1985–86 were observed extensively (Arlot et al. 1989; GSO 1990). This paper presents results of observations made at the Vainu Bappu Observatory during 1985. 70 R. Vasundhara 2. Observations The observations were made using the 102 cm reflector and a single channel photometer at the Vainu Bappu Observatory (VBO). A narrow band filter in the Hα region (continuum) was used on all occasions except on 1985 October 17. Focal plane diaphragms of diameters 9 or 12 arcsec were used. The red region and small aperture ensured significant reduction in the contribution of the sky background. The recording system consisted of an EMI 9658 phototube and a pulse counting unit with a cyclic buffer, which on keyboard operation, wrapped around to order the last 1048 data points. The integration time for each event was selected based on predicted duration so that the entire event could be captured within the 1048 data points. The sky conditions were generally poor on all days except on 1985 October 24. Table 1(a) lists the log of observations. 3. Data reduction 3.1 Determination of the Time of Light Minimum The time of light minimum of the events was determined by finding the value of n for which the condition was satisfied, where the summation was carried out over a span of i points on either side of the trial point n. For each light curve i was selected so as to avoid wings of light curves affected due to the presence of clouds. Column 2 in Table 1(a) gives the observed times of light minimum Tmino. The large uncertainty of ± 25 s for the 1985 November 15 event was due to the broad minimum and poor sky conditions. The observed eclipse depths are given in Table l(b). The counts were binned at intervals of 5–25 s depending on the signal to noise ratio and then normalized. The normalized light curve was fitted with a theoretical light curve to derive the impact parameter and information on the scattering characteristics of the surface of the eclipsed satellite. 3.2 Calculation of the Eclipse Geometry The shape of the light curve depends on the sizes of the two satellites, the impact parameter (y), sizes of the umbral and penumbral cones and the relative velocity of the eclipsed satellite (SAT2) with respect to the eclipsing one (SAT1) projected on to the plane perpendicular to the shadow axis. The radii of cross sections of the umbral (RU ) and the penumbral (RP) cones at the distance of SAT2 and the projected relative velocity (v) were calculated in the following manner. Heliocentric equatorial coordinates of Jupiter were calculated from the heliocentric longitude and latitude of the planet published in the Indian Astronomical Ephemeris Mutual phenomena 71 Table 1a. Observed and predicted midtimes (UT) * Mid umbral time Table 1b. Observed and predicted eclipse depths (1985) based on the DE-200 ephemeris. The satellite positions were computed using the quick loading routine “KODQIK” along with “EPHEM/E3” and “GALSAT” (Lieske 1980). Correction for light travel time was taken into acco.un t by. com. bining the heliocentric equatorial position (Xs1, Ys1, Zs1) and velocity (Xs1, Ys1, Zs1) of the eclipsing satellite at time. Ts1. wh.en light from the Sun reached it, and the position (Xs2, Ys2, Zs2) and velocity (Xs2, Ys2, Zs2) of the eclipsed satellite at time Ts2 when light left it after reflection from its surface towards the observer, reaching him at time Tobs. The 72 R. Vasundhara heliocentric distances and velocities of the satellites were calculated from (1) (2) . where (XJm, YJm, ZJm) and (XJm, YJm, ZJm) are the position and velocity of Jupiter at time Tsm (m = 1, 2). The positions and velocities of the two satellites along Earth’s equatorial coordinates centered at the barycenter of the Jupiter system are (x , y , . sm sm zsm) and (xsm, ysm, zsm) respectively. Ts1 and Ts2 were obtained iteratively from the observed midtime Tobs. The solutions converged within 3 to 4 iterations. The projected relative velocity ν and distance d are given by (3) where θ12 is the angle between the two vectors Rs1 and Rs2, θm the angle between SATm – Sun vector and the direction of motion of the corresponding satellite, and rs1 s2 is the distance (xs1s2, ys1s2, Zs1s2) between the two satellites. The angle u between SAT1 – Sun and SAT1 – SAT2 vectors is given by: (4) The midtimes and impact parameters predicted using this method are given in columns 4–7 of Tables 1(a) and columns 4–6 of 1(b) respectively along with the predictions E-2 and G-5 by Arlot (1984) and AF by Aksnes & Franklin (1984). The impact parameter in column 3 Table 1(b) was calculated from the fitted impact parameter. The radii of cross sections of the umbral and penumbral cones at the distance of the eclipsed satellite were calculated using the following relations (Aksnes 1974): (5) (6) where Rs and R1 are the radii of the Sun and the eclipsing satellite respectively. The radii of Io, Europa and Ganymede were taken to be 1815, 1569 and 2631 kms respectively (Morrison 1982) Mutual phenomena 73 3.3 Computation of Light Loss The light loss in the umbra and the penumbra were computed using the method described by Aksnes & Franklin (1976) but modified to include the effect of limb darkening on the eclipsed satellite. Fig. 1 shows the geometry for a particular case as seen from the Sun. The eclipsed satellite totally encompasses the umbra UU¢ and part of the penumbra (LTIWMKL). Fig. 2 depicts the heliocentric view of SAT2; S2 is the centre of the eclipsed satellite, S and Ε the subsolar and subterrestrial points respectively. The great circle perpendicular to S2 S in the plane ENS2 W is represented as (LTIWMDL) in Fig. 1. The loss in light in the penumbra Lp is given by (7) The intensity in the penumbra 1 – lp (x), at a distance x from the shadow axis was calculated using a method described by Aksnes & Franklin (1976) taking into account the limb darkening on the Sun at the wavelength of observation. is the elementary area at the point Q'(θ, ψ) on the surface of SAT2 of which x dx dφ is the projection on the disc at the point Q as seen from the Sun (Fig. 1). If i and e are the Figure 1. Geometry of eclipse for a particular case when SAT2 totally encompasses the umbra UU' and part of the penumbra PP'. O is the shadow centre and S2 is the centre of SAT2. Motion of SAT2 is along S2S'2. 74 R. Vasundhara Figure 2. Heliocentric view of SAT2. cos(i) = μ0 = cos ψ cos θ, cos (e) = μ1=cos ψ cos(θ + α). The azimuth θ is measured from the subsolar point S in the plane containing centre of SAT2, S and the subterrestrial point E. S2 Ν is parallel to Jupiter’s spin axis. The point Q' on the surface of SAT2 is projected as Q on the disc.
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